The X-ray polarisation of the Seyfert 1 galaxy IC 4329A
A Ingram, M Ewing, A Marinucci, D Tagliacozzo, D J Rosario, A Veledina, D E Kim, F Marin, S Bianchi, J Poutanen, G Matt, H L Marshall, F Ursini, A De Rosa, P-O Petrucci, G Madejski, T Barnouin, L Di Gesu, M Dovčiak, V E Gianolli, H Krawczynski, V Loktev, R Middei, J Podgorny, S Puccetti, A Ratheesh, P Soffitta, F Tombesi, S R Ehlert, F Massaro, I Agudo, L A Antonelli, M Bachetti, L Baldini, W H Baumgartner, R Bellazzini, S D Bongiorno, R Bonino, A Brez, N Bucciantini, F Capitanio, S Castellano, E Cavazzuti, C-T Chen, S Ciprini, E Costa, E Del Monte, N Di Lalla, A Di Marco, I Donnarumma, V Doroshenko, T Enoto, Y Evangelista, S Fabiani, R Ferrazzoli, J A García, S Gunji, J Heyl, W Iwakiri, S G Jorstad, P Kaaret, V Karas, F Kislat, T Kitaguchi, J J Kolodziejczak, F La Monaca, L Latronico, I Liodakis, S Maldera, A Manfreda, A P Marscher, I Mitsuishi, T Mizuno, F Muleri, M Negro, C-Y Ng, S L O’Dell, N Omodei, C Oppedisano, A Papitto, G G Pavlov, A L Peirson, M Perri, M Pesce-Rollins, M Pilia, A Possenti, B D Ramsey, J Rankin, O J Roberts, R W Romani, C Sgrò, P Slane, G Spandre, D A Swartz, T Tamagawa, F Tavecchio, R Taverna, Y Tawara, A F Tennant, N E Thomas, A Trois, S S Tsygankov, R Turolla, J Vink, M C Weisskopf, K Wu, F Xie, S Zane- Space and Planetary Science
- Astronomy and Astrophysics
Abstract
We present an X-ray spectro-polarimetric analysis of the bright Seyfert galaxy IC 4329A. The Imaging X-ray Polarimetry Explorer (IXPE) observed the source for ∼500 ks, supported by XMM-Newton (∼60 ks) and NuSTAR (∼80 ks) exposures. We detect polarisation in the 2–8 keV band with 2.97σ confidence. We report a polarisation degree of 3.3 ± 1.1 per cent and a polarisation angle of 78○ ± 10○ (errors are 1σ confidence). The X-ray polarisation is consistent with being aligned with the radio jet, albeit partially due to large uncertainties on the radio position angle. We jointly fit the spectra from the three observatories to constrain the presence of a relativistic reflection component. From this, we obtain constraints on the inclination angle to the inner disc (<39○ at 99 per cent confidence) and the disc inner radius (<11 gravitational radii at 99 per cent confidence), although we note that modelling systematics in practice add to the quoted statistical error. Our spectro-polarimetric modelling indicates that the 2–8 keV polarisation is consistent with being dominated by emission directly observed from the X-ray corona, but the polarisation of the reflection component is completely unconstrained. Our constraints on viewer inclination and polarisation degree tentatively favour more asymmetric, possibly out-flowing, coronal geometries that produce more highly polarised emission, but the coronal geometry is unconstrained at the 3σ level.